Progenitor mass constraints for core-collapse supernovae from correlations with host galaxy star formation⋆
By Jay Anderson, S. Habergham, P. James, M. Hamuy. 2012
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Using Hemission as a tracer of on-going (<16 Myr old) and near-UV emission as a tracer of recent (16-100 Myr old) star formation, we present constraints on the properties of core- collapse supernova progenitors through the association of their explosion sites with star form- ing regions. Amalgamating previous results with those gained from new data, we present statistics of a large sample of supernovae; 163.5 type II (58 IIP, 13 IIL, 13.5 IIb, 19 IIn and 12 'impostors', plus 48 with no sub-type classification) and 96.5 type Ib/c (39.5 Ib and 52 Ic, plus 5 with no sub-type classification). Using pixel statist ics we build distributions of asso- ciations of different supernova types with host galaxy star formation. Our main findings and conclusions are: 1) An increasing progenitor mass sequence is observed, implied from an increasing associ- ation of supernovae to host galaxy Hemission. This commences with the type Ia showing the weakest association, followed by the type II, then the Ib , with the Ic showing the strongest correlation to star forming regions. Thus our progenitor mass sequence runs Ia-II-Ib-Ic. 2) Overall the type Ibc supernovae are found to occur nearer to bright HII regions than super- novae of type II. This implies that the former have shorter stellar lifetimes thus arising from more massive progenitor stars. 3) While type IIP supernovae do not closely follow the on-going star formation, they accu- rately trace the recent formation. This implies that their p rogenitors arise from stars at the low end of the CC SN mass sequence, consistent with direct detections of progenitors in pre- explosion imaging. 4) Similarly the type IIn supernovae trace recent but not the on-going star formation. This implies that, contrary to the general consensus, the majori ty of these supernovae do not arise from the most massive stars. Results and suggestive constraints are also presented for t he less numerous supernovae of types IIL, IIb, and supernova 'impostors'. Finally we prese nt analysis of possible biases in the data, the results of which argue strongly against any select ion effects that could explain the relative excess of type Ibc supernovae within bright HII regions. Thus intrinsic progenitor dif- ferences in the sense of the mass sequence we propose remain the most plausible explanation of our findings.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/ae5483a6b46b849247ad7690c9dbfbc09c85aa45
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Citations in the corpus
- TYPE Ia SUPERNOVAE STRONGLY INTERACTING WITH THEIR CIRCUMSTELLAR MEDIUM (2013, methodology): “CONCLUSIONS Running SNID on the Berkeley SN Group’s database of SN IIn spectra, we have reidentified four SNe IaCSM that were previously known (SNe 2008J, 2008cg, 25 Note that none of the SNe Ia-CSM discussed herein were part of the Anderson et al. (2012) sample.”
- Spectroscopy of superluminous supernova host galaxies. A preference of hydrogen-poor events for extreme emission line galaxies (2014, background): “UV light probes recent (16–100 Myr) star formation, while Hα is sensitive to the ongoing SF over shorter time-scales (e.g. Anderson et al. 2012).”
- Observational Constraints on the Progenitors of Core-Collapse Supernovae: The Case for Missing High-Mass Stars (2015, background): “Anderson et al. (2012) and Anderson & James (2008) have matched the positions of nearby SNe to the Hα emission produced in star-forming regions.”
- Bolometric light curves and explosion parameters of 38 stripped-envelope core-collapse supernovae (2014, background): “…SN locations within the hosts (e.g. Anderson & James 2008; Boissier & Prantzos 2009; Anderson et al. 2010; Leloudas et al. 2011; Modjaz et al. 2011; Anderson et al. 2012; Kelly & Kirshner 2012; Crowther 2013), the stellar populations surrounding SNe (e.g. Kuncarayakti et al. 2013; Williams et al.…”
- Luminous blue variables are antisocial: their isolation implies that they are kicked mass gainers in binary evolution (2014, background): “As noted in the introduction, Anderson and collaborators (Anderson & James 2009; Anderson et al. 2012; Habergham et al. 2014) have found that SN IIn show a weaker association with Hα emission in host galaxies, as compared to SNe Ibc, and their Hα association is closer to that of SNe II-P (or…”
- Carnegie Supernova Project: Observations of Type IIn supernovae ⋆ (2013, background): “Interestingly, Anderson et al. (2012) showthat SNe IIn are located in environments similar to those of SNe IIP (whose progenitors are RSGs), indicating that the majorityof events may not arise from very massive stars like LBVs.”
- OPTICAL SPECTRA OF 73 STRIPPED-ENVELOPE CORE-COLLAPSE SUPERNOVAE (2014, background): “Specifically, SNe Ib and SNe Ic appear to trace differently their respective host galaxy’s distributions of Hα emission (Anderson & James 2008; Anderson et al. 2012) and the brightest blue regions (Kelly et al. 2008; Kelly & Kirshner 2012), with SNe Ic having higher correlations with both…”
- CHARACTERIZING THE V-BAND LIGHT-CURVES OF HYDROGEN-RICH TYPE II SUPERNOVAE (2014, methodology): “This picture is also supported by work on the environments of CC SNe, where SNe IIL show a higher degree of association to host galaxy on-going star formation (as traced by Hα emission) than their SNe IIP counterparts (Anderson et al. 2012).”